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A Global View of Molecule-Forming Clouds in the Galaxy

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Steven J. Gibson ,
Ward S. Howard ,
Christian S. Jolly ,
Jonathan H. Newton ,
Aaron C. Bell ,
Mary E. Spraggs ,
J. Marcus Hughes ,
Aaron M. Tagliaboschi ,
Christopher M. Brunt  and
A. Russell Taylor
...Show all authors
Steven J. Gibson
Affiliation:
Western Kentucky U.
Ward S. Howard
Affiliation:
Western Kentucky U. Union U. U. North Carolina-Chapel Hill
Christian S. Jolly
Affiliation:
Western Kentucky U. C. M. Gatton Acad.
Jonathan H. Newton
Affiliation:
Western Kentucky U. McMaster U.
Aaron C. Bell
Affiliation:
Western Kentucky U. U. Tokyo
Mary E. Spraggs
Affiliation:
Western Kentucky U. C. M. Gatton Acad.
J. Marcus Hughes
Affiliation:
Western Kentucky U. C. M. Gatton Acad.
Aaron M. Tagliaboschi
Affiliation:
Western Kentucky U.
Christopher M. Brunt
Affiliation:
Exeter U.
A. Russell Taylor
Affiliation:
U. Calgary U. Cape Town
Jeroen M. Stil
Affiliation:
U. Cape Town
Thomas M. Dame
Affiliation:
Harvard-CfA
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Abstract

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We have mapped cold atomic gas in 21cm line H i self-absorption (HISA) at arcminute resolution over more than 90% of the Milky Way's disk. To probe the formation of H2 clouds, we have compared our HISA distribution with CO J = 1-0 line emission. Few HISA features in the outer Galaxy have CO at the same position and velocity, while most inner-Galaxy HISA has overlapping CO. But many apparent inner-Galaxy HISA-CO associations can be explained as chance superpositions, so most inner-Galaxy HISA may also be CO-free. Since standard equilibrium cloud models cannot explain the very cold H i in many HISA features without molecules being present, these clouds may instead have significant CO-dark H2.

Keywords

radiative transfersurveysstars: formationISM: cloudsISM: evolutionISM: moleculesGalaxy: kinematics and dynamicsGalaxy: structureradio lines: ISM
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , E27
Copyright
Copyright © International Astronomical Union 2016 

References

Dame, T. M. et al. 2001, ApJ, 547, 792 CrossRefGoogle Scholar
Gibson, S. J. 2010, ASP-CS, 438, 111 Google Scholar
Gibson, S. J., et al. 2005b, ApJ, 626, 214 CrossRefGoogle Scholar
Gibson, S. J., et al. 2005a, ApJ, 626, 195 CrossRefGoogle Scholar
Gibson, S. J., et al. 2000, ApJ, 540, 851 CrossRefGoogle Scholar
Heyer, M. H., et al. 1998, ApJS, 115, 241 Google Scholar
Jackson, J. M., et al. 2006, ApJS, 163, 145 CrossRefGoogle Scholar
McClure-Griffiths, N. M., et al. 2005, ApJS, 158, 178 CrossRefGoogle Scholar
Sanders, D. B., et al. 1986, ApJS, 60, 1 Google Scholar
Stil, J. M., et al. 2006, AJ, 132, 1158 Google Scholar
Taylor, A. R., et al. 2003, AJ, 125, 3145 CrossRefGoogle Scholar
Taylor, J. H., & Cordes, J. M. 1993, ApJ, 411, 674 Google Scholar
Wolfire, M. G., et al. 2010, ApJ, 716, 1191 CrossRefGoogle Scholar
Wolfire, M. G., et al. 2003, ApJ, 587, 278 Google Scholar